The intrinsic Baldwin effect in broad Balmer lines of six long-term monitored AGNs

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Volume 603 (July 2017)

A&A, 603 (2017) A49

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Table 1

Basic information about the observations of the used spectra.

Object^a	Type^b	Period^c	Telescope^d	Aperture^e	Line^f	Continuum^g	No.^h	Referenceⁱ

NGC 5548	Seyfert 1	1996–2002	SAO, GHAO, OAN-SPM	4.2′′ × 19.8′′	Hα	5100 Å	23	1
					Hβ	5100 Å	81
NGC 4151	Seyfert 1	1996–2006	SAO, GHAO, OAN-SPM	2.0′′ × 6.0′′	Hα	5100 Å	137	2
					Hβ	5100 Å	181
3C 390.3	DPL	1995–2007	SAO, GHAO, OAN-SPM	2.0′′ × 6.0′′	Hβ	5100 Å	128	3
Arp 102B	DPL	1987–2013	SAO, GHAO, OAN-SPM, CA	2.5′′ × 6.0′′	Hα	6200 Å	88	4
					Hβ	5100 Å	116
Ark 564	NLSy1	1999–2010	SAO, GHAO, OAN-SPM	2.5′′ × 6.0′′	Hα	6200 Å	50	5
					Hβ	5100 Å	91
E1821+643	quasar	1990–2014	SAO, GHAO, CA	2′′ × 6.0′′	Hβ	5100 Å	127	6

Notes.Columns:

^(a)

Object name;

^(b)

AGN type;

^(c)

Monitored period;

^(d)

Telescope used (SAO – 6 m and 1m telescopes of Special Astrophysical Observatory; GHAO – 2.1 m telescope of Guillermo Haro Astrophysical Observatory; OAN-SPM – 2.1 m telescope of the Observatorio Astronómico Nacional at San Pedro Martir; and CA – 3.5 m and 2.2 m telescopes of Calar Alto);

^(e)

Projected spectrograph entrance apertures (slit width×slit length in arcsec);

^(f)

E mission line;

^(g)

Continuum;

^(h)

Number of spectra;

⁽ⁱ⁾

Reference from which line and continuum fluxes are taken.

Reference. (1) Shapovalova et al. (2004); (2) Shapovalova et al. (2008); (3) Shapovalova et al. (2010a); (4) Shapovalova et al. (2013); (5) Shapovalova et al. (2012); (6) Shapovalova et al. (2016).

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